J/A+A/579/A102 Hα imaging of Herschel Reference Survey (Boselli+, 2015)
Hα imaging of the Herschel Reference Survey. The star formation properties
of a volume-limited, K-band-selected sample of nearby late-type galaxies.
Boselli A., Fossati M., Gavazzi G., Ciesla L., Buat V., Boissier S.,
Hughes T.
<Astron. Astrophys. 579, A102 (2015)>
=2015A&A...579A.102B 2015A&A...579A.102B
ADC_Keywords: Galaxy catalogs ; Photometry, H-alpha ; Equivalent widths ;
Morphology ; Spectroscopy
Keywords: galaxies: spiral - galaxies: star formation -
galaxies: fundamental parameters - galaxies: clusters: general -
galaxies: photometry - galaxies: luminosity function, mass function
Abstract:
We present new Hα+[NII] imaging data of late-type galaxies in
the Herschel Reference Sample aimed at studying the star formation
properties of a K-band-selected, volume-limited sample of nearby
galaxies. The Hα+[NII] data are corrected for [NII]
contamination and dust attenuation using different recipes based on
the Balmer decrement and the 24um luminosities. We show that the
Hα luminosities derived with different corrections give
consistent results only whenever the the uncertainty on the estimate
of the Balmer decrement is [C(Hβ)]≤0.1. We use these data to
derive the star formation rate of the late-type galaxies of the
sample, and compare these estimates to those determined using
independent monochromatic tracers (FUV, radio continuum) or the output
of spectral energy distribution (SED) fitting codes. This comparison
suggests that the 24um based dust extinction correction for the
Hα data might be non universal, and that it should be used with
caution in all objects with a low star formation activity, where dust
heating can be dominated by the old stellar population. Furthermore,
because of the sudden truncation of the star formation activity of
cluster galaxies occurring after their interaction with the
surrounding environment, the stationarity conditions required to
transform monochromatic fluxes into star formation rates might not
always be satisfied in tracers other than the Hα luminosity. In
a similar way, the parametrisation of the star formation history
generally used in SED fitting codes might not be adequate for these
recently interacting systems. We then use the derived star formation
rates to study the SFR luminosity distribution and the typical scaling
relations of the late-type galaxies of the HRS. We observe a
systematic decrease of the specific star formation rate with
increasing stellar mass, stellar mass surface density, and
metallicity. We also observe an increase of the asymmetry and
smoothness parameters measured in the Hα-band with increasing
SSFR, probably induced by an increase of the contribution of giant HII
regions to the Hα luminosity function in star-forming
low-luminosity galaxies.
Description:
We present the Tables containing the data relative to the Halpha+[NII]
observations and the derived parameters for the Herschel Reference
Survey.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 130 323 The Herschel Reference Survey (HRS)
table2.dat 56 148 Hα observational parameters of the
138 target galaxies
table3.dat 43 323 Hα+[NII] fluxes and equivalent widths
table4.dat 58 218 CAS parameters for the HRS galaxies
table5.dat 24 323 Radio continuum data
table6.dat 60 236 Star formation rates
table7.dat 64 264 Fluxes of the emission lines normalised to
Hα determined using GANDALF
refs.dat 77 24 References
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See also:
J/PASP/122/261 : Herschel Reference Survey Sample (Boselli+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- HRS [1/323] HRS name <[BEC2010] HRS NNN> in Simbad
5- 10 I6 --- CGCG ?=- CGCG (Cat. VII/190) name
12- 15 I4 --- VCC ?=- VCC (Cat. J/AJ/90/1681) name
17- 20 I4 --- UGC ?=- UGC (Cat. VII/26) name
22- 25 I4 --- NGC ?=- NGC (Cat. VII/118) name
26 A1 --- m_NGC [A] Multiplicity index on NGC
28- 31 I4 --- IC ?=- IC (Cat. VII/118) name
33- 34 I2 h RAh Right Ascension (J2000.0)
36- 37 I2 min RAm Right Ascension (J2000.0)
39- 43 F5.2 s RAs Right Ascension (J2000.0)
45 A1 --- DE- Declination sign (J2000.0)
46- 47 I2 deg DEd Declination (J2000.0)
49- 50 I2 arcmin DEm Declination (J2000.0)
52- 55 F4.1 arcsec DEs Declination (J2000.0)
57- 76 A20 --- MType Morphological type
77- 82 F6.2 Mpc Dist [15/172] Distance (1)
84- 88 F5.2 [Msun] logM* [8.4/11.6]?=- Stellar mass (2)
89 A1 --- n_logM* [a] Method used to derive logM* (2)
91- 95 F5.2 arcmin D24.5g [0.5/13] g-band diameter (3)
97-101 F5.2 deg Incl [0/90] Inclination (4)
103-107 I5 km/s Vel [-273/12000] Recessional velocity (5)
109-128 A20 --- Memb Cluster or cloud membership (6)
130 I1 --- Ha [0/1] Hα data available ? 1=yes, 0=no
-------------------------------------------------------------------------------
Note (1): Distances have been determined from the recessional velocity assuming
a Hubble constant H0=70km/s/Mpc for galaxies outside the Virgo cluster, and
assumed to be 17Mpc for galaxies belonging to Virgo, with exception to those
located in the Virgo cluster B substructure (23Mpc; Gavazzi et al.,
1999MNRAS.304..595G 1999MNRAS.304..595G).
Note (2): Stellar mass, from Cortese et al. 2012 (J/A+A/544/A101), determined
following the prescription of Zibetti et al. (2009MNRAS.400.1181Z 2009MNRAS.400.1181Z) based on
the i-band luminosity and g-i mass-to-light ratio.
For galaxies without SDSS g and i-band data (11 objects, marked with 'a'),
stellar masses have been computed using the prescription of Boselli et al.
(2009ApJ...706.1527B 2009ApJ...706.1527B) based on the H-band luminosity and B-H mass-to-light
ratio.
Note (3): g-band optical isophotal diameter (24.5mag/arcsec2), from Cortese
et al. 2012 (J/A+A/544/A101). For the HRS galaxies without SDSS images, the
g-band isophotal diameter was determined from the relation given in NED
(Boselli et al. 2014, J/A+A/564/A65):
r24.5(g) = 0.871(±0.017)r25(B) + 6.041(±2.101)
Note (4): inclination of the galaxy, determined using the prescription based on
the morphological type described in Haynes & Giovanelli (1984AJ.....89..758H 1984AJ.....89..758H)
and the i-band ellipticity given in Cortese et al. 2012 (J/A+A/544/A101).
Note (5): from HI data when available (Boselli et al., 2014, J/A+A/564/A65),
otherwise from NED.
Note (6): from Gavazzi et al. (1999MNRAS.304..595G 1999MNRAS.304..595G) for Virgo and
Tully (1987ApJ...321..280T 1987ApJ...321..280T) or Nolthenius (1993ApJS...85....1N 1993ApJS...85....1N) whenever
available, or from our own estimate (Boselli et al., 2010, J/PASP/122/261).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS galaxy name
5- 8 I4 0.1nm Filter [6570/6607] ON-band filter wavelength
10- 12 F3.1 m Tel Telescope size
14- 17 A4 --- CCD Used CCD
19- 22 F4.2 arcsec Size [0.28/0.35] Pixel size
24- 27 I4 yr Year [2006/2012] Year of the observations
29 I1 --- Nexp [1/5] Number of exposures
31- 36 F6.1 s Texp [180/1200] ON-band exposure time per pose
38- 41 F4.2 --- AirM [1/1.8] Air mass
43 I1 --- Phot [0/1] Photometric quality of the sky, i=good (1)
45- 50 F6.2 mW/m2 Zp [-15.8/-14.6]?=- Zero point of the observation
52- 56 F5.3 --- n [0.09/1.8] Normalisation factor between the
ON- and the OFF-band (r-Gunn) filter
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Note (1): Photometric quality of the sky flag as follows:
1 = photometric conditions
0 = unclear conditions (thin cirrus)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS name
5- 6 I2 0.1nm EW [-2/78]?=- Hα+[NII] equivalent width
8- 9 I2 0.1nm e_EW [0/36]?=- error on the EWHa+[NII]
11- 16 F6.2 [mW/m2] logF [-13.81/-10.85]?=- Hα+[NII] flux
17 A1 --- u_logF Uncertainty flag on logF(Ha+[NII])
19- 22 F4.2 [mW/m2] e_logF [0.02/1]?=- Error on logF(Hal+[NII])
23 A1 --- f_logF [:] Uncertainty flag on e_logF(Ha+[NII])
25- 29 A5 --- Ref Reference, in refs.dat file
31- 41 A11 --- Ref2 Alternative reference, in refs.dat file
43 A1 --- n_logF [cmv] Notes on Hα+[NII] fluxes (7)
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Note (7): Notes as follows:
c = the flux of the galaxy has been determined by indirectly calibrating
the image using the published flux of the companion galaxy
m = the published value is a mean value of two independent measurements
v = vignetted images where the total flux cannot be properly extracted
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS name
5- 10 F6.2 arcsec re(r) [3/136]?=- r band effective radius re(r)
12- 17 F6.2 arcsec re(Ha) [2.6/144]?=- Hα+[NII] effective radius
19- 24 F6.2 arcsec re(EW) [5/211]?=- Hα+[NII] equivalent width
effective radius
26- 29 F4.2 --- Cr [1.9/5.2] r band concentration index
31- 35 F5.2 --- Ar [-0.1/0.4] r band asymmetry
37- 41 F5.2 --- Sr [-0.1/1.2] r band clumpiness
43- 46 F4.2 --- CH [0.2/5.6]?=- Hα+[NII] concentration index
48- 52 F5.2 --- AH [-0.17/1]?=- Hα+[NII] asymmetry
54- 58 F5.2 --- SH [-1.1/2.21]?=- Hα+[NII] clumpiness
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS name
5 I1 --- f_S20 [0/2] code for detections (1) and
undetections (0) of 20cm data
7- 14 F8.1 mJy S20 [0.2/266000] Radio flux density at 20cm
or upper limit
16- 20 F5.2 [W/Hz] logL20 [18/25] Radio luminosity at 20cm or upper limit
22 I1 --- q_S20 [1/2]?=- 20cm data quality: 1=high, 2=uncertain
24 I1 --- r_S20 [1/6] Reference (8)
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Note (8): References as follows:
1 = Condon et al. (1990ApJS...73..359C 1990ApJS...73..359C, Cat. J/ApJS/73/359)
2 = Condon (1987ApJS...65..485C 1987ApJS...65..485C, Cat. J/ApJS/65/485)
3 = Condon et al. (1987ApJS...65..543C 1987ApJS...65..543C)
4 = Condon et al. (2002AJ....124..675C 2002AJ....124..675C)
5 = extracted as described in the text from the NVSS survey
(Condon et al., 1998AJ....115.1693C 1998AJ....115.1693C,, Cat. VIII/65)
6 = extracted from the FIRST survey (Becker et al., 1995ApJ...450..559B 1995ApJ...450..559B,
Cat. VIII/90)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS name
5- 10 F6.4 Msun/yr SFR1 ?=- Star formation rate determined using
Hα data corrected for attenuation
using the Balmer decrement
12- 17 F6.4 Msun/yr SFR2 ?=- Star formation rate determined using
Hα data corrected for attenuation
using the 24um emission
19- 24 F6.4 Msun/yr SFR3 ?=- Star formation rate determined using
FUV emission corrected for attenuation
using the 24um emission
26- 32 F7.4 Msun/yr SFR4 ?=- Star formation rate determined using the
radio 20cm emission
34- 39 F6.4 Msun/yr SFRm [0.01/9.3]?=- Star formation rate determined by
averaging the previous 4 estimates
41- 46 F6.4 Msun/yr SFR6 ?=- Star formation rate determined using SED
fitting with 1 exponentially declining SFR
48- 53 F6.4 Msun/yr SFR7 ?=- Star formation rate determined using SED
fitting with 2 exponentially declining SFR
55- 60 F6.4 Msun/yr SFR8 ?=- Star formation rate determined using SED
fitting with a delaied SFR
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] HRS name
5- 8 F4.2 --- F3727 ?=- [OII]3727 flux normalised to Hα
10- 13 F4.2 --- FHb ?=- Hβ flux normalised to Hα
15- 18 F4.2 --- F5007 ?=- [OIII]5007 flux normalised to Hα
20- 23 F4.2 --- FHa [1]?=- Hα flux normalised to Hα
25- 28 F4.2 --- F6584 ?=- [NII]6584 flux normalised to Hα
30- 33 F4.2 --- F6716 ?=- [SII]6716 flux normalised to Hα
35- 38 F4.2 --- F6731 ?=- [SII]6731 flux normalised to Hα
40- 45 F6.2 --- S/Na ?=- Signal-to-noise at Hα
47- 52 F6.2 --- S/Nb ?=- Signal-to-noise at Hβ
54- 58 F5.2 --- C(Hb) ?=- Balmer decrement
60- 64 F5.2 --- e_C(Hb) ?=- Error on the Balmer decrement
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Ref Reference code
4- 22 A19 --- BibCode BibCode
24- 55 A32 --- Aut Author's name
57- 77 A21 --- Com Comments
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Acknowledgements:
Alessamdro Boselli, alessandro.boselli(at)lam.fr
(End) Patricia Vannier [CDS] 09-Apr-2015